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4.1.1.4 Solar photosphere and chromosphere
Continuum surface intensity (λ 4364.00 Å)
δIrms= 25.4 %
10
10
8
y [Mm]
8
y [Mm]
6
6
4
4
2
2
0
0
0
0
2
4
6
x [Mm]
8
2
4
10
6
x [Mm]
8
10
y [arcsec]
μ = 1.0
μ = 0.8
μ = 0.6
μ = 0.4
μ = 0.2
brightness temperature at λ = 1.0 mm [103 K]
Fig. 12. Left: Quiet solar granulation as observed with the 1m Swedish Solar Telescope (courtesy Mats Carlsson
2004). Right: High-resolution CO5BOLD simulation of solar surface convection on a nx × ny × nz = 400 × 400 × 165
grid. Both images show the emergent continuum intensity (using identical scaling) at λ 436.4 nm in a field measuring
15´´ × 15´´ (11 × 11 Mm). Reproduced from [07Ste1].
7.0
6
6
6
6
6
4
4
4
4
4
5.0
2
2
2
2
2
4.0
0
3.0
0
0
0
1
2
3
4
5
x [arcsec]
6
7
0
0
1
2
3
4
x [arcsec]
5
6
0
0
1
2
3
x [arcsec]
4
0
1
2
x [arcsec]
3
6.0
0
1
x [arcsec]
Fig. 19. Top: Gas temperature at a geometric height of z = 1000 km above τRoss = 1 in the nonmagnetic 3D
chromospheric model by [04Wed]. Temperatures range from 2000 K (black) to 7000 K (white). Bottom: Brightness
temperature Tb of synthetic continuum images at λ 1 mm, computed from the snapshot shown at left for different
inclination angles (μ = 1: disk-center, μ = 0.2: close to limb). Tb ranges from 3000 K (black) to 7000 K (white).
Adapted from [07Wed3].
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moss
hot plasma
corona
canopy domain
le I
chromosphere
E
canopy domain
C
fib
ril
D
cs = cA
fibr
il
spic
u
~1.5 Mm
spic
ule II
Al
fv
én
wa
ve
s
transition region
F
sub-canopy domain
fluctosphere
~1 Mm
sub-canopy
domain
fluctosphere
shock waves
current sheets
weak fields
A
~0.5 Mm classical temperature
minimum
small-scale canopies / HIFs
B
reversed granulation
photosphere
0 Mm
τ500 = 1
convection
zone
granulation
network
p-modes / g-modes
internetwork
network
}
supergranulation
network
Wedemeyer-Böhm et al. (2008)
Fig. 20. Schematic, simplified structure of the lower atmosphere of the quiet Sun (dimensions not to scale).
Reproduced from [08Wed1].
4.1.1.5 Solar transition region and quiet corona
Fig. 6. A small coronal hole seen on the solar disk in the Mg IX (70.6 nm) line (middle panel). In the continuum near
71 nm (on the left) the magnetic network structure is the same inside and outside the coronal hole. The Doppler
image shows LOS velocities of ±30 km s−1 with outflows (blue shifts) in the hole area.
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4.1.2 Solar activity
4.1.2.1 Active regions
Fig. 2. Moss region
observed in the 17.1 nm
wavelength band on 6
June 1999. The square
box with an angular size
of 19´´ × 19´´ contains
bright moss structures
with
a
brightness
distribution given in the
histogram inset. AR loops
can be seen in the
neighbourhood
(from
[00Mar]).
4.1.2.2 Solar activity cycle
Fig. 5. Butterfly
diagram of the
radial component of the solar
magnetic field
[03Hat].
For
each Carrington
rotation,
the
magnetic flux is
summed in longitude in each
latitude bin.
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4.1.2.3 Sun spots
Fig. 1. Image of a complex sunspot with two
umbrae observed in the red continuum with the
Swedish Solar Telescope on La Palma. With kind
permission of J. Hirzberger.
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4.1.2.5 Prominences and ejecta
Fig 2. Spicule activity at the solar limb in O V emission at 62.973 nm with the corresponding Doppler diagram in the
lower panel. The frame dimensions are 310 Mm × 100 Mm. The tallest feature protrudes approximately 40 Mm from
the limb and is a macrospicule judged by its length. The size of the Earth is shown for comparison in the upper panel.
4.2 The planets and their satellites
4.2.1 Introduction
Fig. 1. The eight planets Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune are shown with their
correct relative sizes (the distances are not to scale). The compilation also includes the dwarf planet Pluto and its
moon Charon. The dark spot on Jupiter is the shadow of Io, one of the four Galilean Moons.©C.J. Hamilton
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4.2.3 Terrestrial planets and satellites
4.2.3.1 Geodetic and geophysical data
(a)
Venus
(b)
Radius − 6051.8 [km]
Mars
Radius − 3396 [km]
Moon
(c)
Radius − 1737.4 [km]
Fig. 2. Planetary radii models of Venus, Mars and the Moon. All images are in a Hammer projection with a central
meridian of 0° W. The values are referenced to a sphere of radius 6051.8, 3396 and 1737.4 km for Venus, Mars and
the Moon, respectively. Note the data gaps for Venus and the rotational flattening present for Mars.
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Fig. 3. Radial gravity anomaly gr and geoid height N for the Earth, Venus, Mars and the Moon. All images are in a
Hammer projection with a central meridian of 0° W. (a)-(b) gr and N for the Earth, evaluating the model EIGENGL04C [08För] at a reference radius Rp = 6378.13 km and setting the zonal degree-2 term C20 to zero. (c)-(d) gr and
N for Venus, evaluating the model SHGJ180 [06Rap] at Rp = 6051 km (e)-(f) gr and N for Mars, evaluating the model
MGS95J [05Tyl] at Rp = 3396 km and setting the zonal degree-2 term C20 to zero. (g)-(h) gr and N for the Moon,
evaluating the model LP165P [97Lem] at Rp = 1738 km and setting the zonal degree-2 term C20 and C22 to zero.
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